Model calculations of the evolution of orbits near the 1:3 commensurability with Jupiter

Details Model calculations of the evolution of orbits near the 1:3 commensurability with Jupiter Model calculations of the evolution of orbits near the 1:3 commensurability with Jupiter

Dec 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979pazh....5..669s&link_type=abstract

Pis'ma Astronomicheskii Zhurnal, vol. 5, Dec. 1979, p. 669-673.) Soviet Astronomy Letters, vol. 5, Nov.-Dec. 1979, p. 358-360. T

Astronomy and Astrophysics

Astronomy

1

Jupiter (Planet), Mathematical Models, Orbital Mechanics, Particle Motion, Planetary Orbits, Eccentric Orbits, Evolution (Development), Mass, Spin Resonance, Time Dependence, Two Body Problem

Scientific paper

Model calculations over a time span of about 500 yr show that mass points initially traveling in orbits whose major semiaxis a(0) = 2.5004 AU will oscillate about its inital value with an amplitude depending strongly on the starting position of the mass point in its orbit. The width of the zone of resonance motion, as defined by the maximum amplitude of the a oscillations, increases with the eccentricity of the original orbit. Among orbits having an initial a(0) in the neighborhood of a = 2.5004 AU but which are confined inside the resonance zone, at least some will be drawn by Jupiter into oscillations about the value a = 2.5004 AU.

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